The hard X-ray imager (HXI) onboard ASTRO-H

The HXI team

    Research output: Chapter in Book/Report/Conference proceedingConference contribution

    13 Citations (Scopus)

    Abstract

    Hitomi X-ray observatory launched in 17 February 2016 had a hard X-ray imaging spectroscopy system made of two hard X-ray imagers (HXIs) coupled with two hard X-ray telescopes (HXTs). With 12 m focal length, they provide fine (2′ half-power diameter; HPD) imaging spectroscopy at 5 to 80 keV. The HXI main imagers are made of 4 layers of Si and a CdTe semiconductor double-sided strip detectors, stacked to enhance detection efficiency as well as to enable photon interaction-depth sensing. Active shield made of 9 BGO scintillators surrounds the imager to provide with low background. Following the deployment of the Extensible Optical Bench (EOB) on 28 February, the HXI was gradually turned on. Two imagers successfully started observation on 14 March, and was operational till the incident lead to Hitomo loss, on 26 March. All detector channels, 1280 ch of imager and 11 channel of active shields and others each, worked well and showed performance consistent with those seen on ground. From the first light observation of G21.5-0.9 and the following Crab observations, 5-80 keV energy coverage and good detection efficiency were confirmed. With blank sky observations, we checked our background level. In some geomagnetic region, strong background continuum, presumably caused by trapped electron with energy ∼100 keV, is seen. But by cutting the high-background time-intervals, the background became significantly lower, typically with 1-3 × 10-4 counts s-1 keV-1 cm-2 (here cm2 is shown with detector geometrical area). Above 30 keV, line and continuum emission originating from activation of CdTe was significantly seen, though the level of 1-4 × 10-4 counts s-1 keV-1 cm-2 is still comparable to those seen in NuSTAR. By comparing the effective area and background rate, preliminary analysis shows that the HXI had a statistical sensitivity similar to NuSTAR for point sources, and more than twice better for largely extended sources.

    Original languageEnglish
    Title of host publicationSpace Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray
    PublisherSPIE
    Volume9905
    ISBN (Electronic)9781510601895
    DOIs
    Publication statusPublished - 2016
    EventSpace Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray - Edinburgh, United Kingdom
    Duration: 2016 Jun 262016 Jul 1

    Other

    OtherSpace Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray
    CountryUnited Kingdom
    CityEdinburgh
    Period16/6/2616/7/1

    Fingerprint

    Hard X-ray
    Imager
    Image sensors
    X rays
    x rays
    Imaging Spectroscopy
    CdTe
    Detector
    Detectors
    detectors
    Count
    Continuum
    continuums
    Spectroscopy
    crabs
    X-ray Telescopes
    Imaging techniques
    X-ray Imaging
    blanks
    Scintillator

    Keywords

    • active-shield
    • APD
    • BGO
    • CdTe-DSD
    • DSSD
    • Hard X-ray Imager
    • Hitomi
    • in-orbit performance

    ASJC Scopus subject areas

    • Electronic, Optical and Magnetic Materials
    • Condensed Matter Physics
    • Computer Science Applications
    • Applied Mathematics
    • Electrical and Electronic Engineering

    Cite this

    The HXI team (2016). The hard X-ray imager (HXI) onboard ASTRO-H. In Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray (Vol. 9905). [990511] SPIE. https://doi.org/10.1117/12.2231176

    The hard X-ray imager (HXI) onboard ASTRO-H. / The HXI team.

    Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray. Vol. 9905 SPIE, 2016. 990511.

    Research output: Chapter in Book/Report/Conference proceedingConference contribution

    The HXI team 2016, The hard X-ray imager (HXI) onboard ASTRO-H. in Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray. vol. 9905, 990511, SPIE, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, Edinburgh, United Kingdom, 16/6/26. https://doi.org/10.1117/12.2231176
    The HXI team. The hard X-ray imager (HXI) onboard ASTRO-H. In Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray. Vol. 9905. SPIE. 2016. 990511 https://doi.org/10.1117/12.2231176
    The HXI team. / The hard X-ray imager (HXI) onboard ASTRO-H. Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray. Vol. 9905 SPIE, 2016.
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    abstract = "Hitomi X-ray observatory launched in 17 February 2016 had a hard X-ray imaging spectroscopy system made of two hard X-ray imagers (HXIs) coupled with two hard X-ray telescopes (HXTs). With 12 m focal length, they provide fine (2′ half-power diameter; HPD) imaging spectroscopy at 5 to 80 keV. The HXI main imagers are made of 4 layers of Si and a CdTe semiconductor double-sided strip detectors, stacked to enhance detection efficiency as well as to enable photon interaction-depth sensing. Active shield made of 9 BGO scintillators surrounds the imager to provide with low background. Following the deployment of the Extensible Optical Bench (EOB) on 28 February, the HXI was gradually turned on. Two imagers successfully started observation on 14 March, and was operational till the incident lead to Hitomo loss, on 26 March. All detector channels, 1280 ch of imager and 11 channel of active shields and others each, worked well and showed performance consistent with those seen on ground. From the first light observation of G21.5-0.9 and the following Crab observations, 5-80 keV energy coverage and good detection efficiency were confirmed. With blank sky observations, we checked our background level. In some geomagnetic region, strong background continuum, presumably caused by trapped electron with energy ∼100 keV, is seen. But by cutting the high-background time-intervals, the background became significantly lower, typically with 1-3 × 10-4 counts s-1 keV-1 cm-2 (here cm2 is shown with detector geometrical area). Above 30 keV, line and continuum emission originating from activation of CdTe was significantly seen, though the level of 1-4 × 10-4 counts s-1 keV-1 cm-2 is still comparable to those seen in NuSTAR. By comparing the effective area and background rate, preliminary analysis shows that the HXI had a statistical sensitivity similar to NuSTAR for point sources, and more than twice better for largely extended sources.",
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    author = "{The HXI team} and Kazuhiro Nakazawa and Goro Sato and Motohide Kokubun and Teruaki Enoto and Yasushi Fukazawa and Kouichi Hagino and Atsushi Harayama and Katsuhiro Hayashi and Jun Kataoka and Junichiro Katsuta and Philippe Laurent and Francois Lebrun and Olivier Limousin and Kazuo Makishima and Tsunefumi Mizuno and Kunishiro Mori and Takeshi Nakamori and Toshio Nakano and Hirofumi Noda and Hirokazu Odaka and Masanori Ohno and Masayuki Ohta and Shinya Saito and Rie Sato and Hiroyasu Tajima and Hiromitsu Takahashi and Tadayuki Takahashi and Shin'ichiro Takeda and Yukikatsu Terada and Hideki Uchiyama and Yasunobu Uchiyama and Shin Watanabe and Kazutaka Yamaoka and Yoichi Yatsu and Takayuki Yuasa",
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    AU - Kokubun, Motohide

    AU - Enoto, Teruaki

    AU - Fukazawa, Yasushi

    AU - Hagino, Kouichi

    AU - Harayama, Atsushi

    AU - Hayashi, Katsuhiro

    AU - Kataoka, Jun

    AU - Katsuta, Junichiro

    AU - Laurent, Philippe

    AU - Lebrun, Francois

    AU - Limousin, Olivier

    AU - Makishima, Kazuo

    AU - Mizuno, Tsunefumi

    AU - Mori, Kunishiro

    AU - Nakamori, Takeshi

    AU - Nakano, Toshio

    AU - Noda, Hirofumi

    AU - Odaka, Hirokazu

    AU - Ohno, Masanori

    AU - Ohta, Masayuki

    AU - Saito, Shinya

    AU - Sato, Rie

    AU - Tajima, Hiroyasu

    AU - Takahashi, Hiromitsu

    AU - Takahashi, Tadayuki

    AU - Takeda, Shin'ichiro

    AU - Terada, Yukikatsu

    AU - Uchiyama, Hideki

    AU - Uchiyama, Yasunobu

    AU - Watanabe, Shin

    AU - Yamaoka, Kazutaka

    AU - Yatsu, Yoichi

    AU - Yuasa, Takayuki

    PY - 2016

    Y1 - 2016

    N2 - Hitomi X-ray observatory launched in 17 February 2016 had a hard X-ray imaging spectroscopy system made of two hard X-ray imagers (HXIs) coupled with two hard X-ray telescopes (HXTs). With 12 m focal length, they provide fine (2′ half-power diameter; HPD) imaging spectroscopy at 5 to 80 keV. The HXI main imagers are made of 4 layers of Si and a CdTe semiconductor double-sided strip detectors, stacked to enhance detection efficiency as well as to enable photon interaction-depth sensing. Active shield made of 9 BGO scintillators surrounds the imager to provide with low background. Following the deployment of the Extensible Optical Bench (EOB) on 28 February, the HXI was gradually turned on. Two imagers successfully started observation on 14 March, and was operational till the incident lead to Hitomo loss, on 26 March. All detector channels, 1280 ch of imager and 11 channel of active shields and others each, worked well and showed performance consistent with those seen on ground. From the first light observation of G21.5-0.9 and the following Crab observations, 5-80 keV energy coverage and good detection efficiency were confirmed. With blank sky observations, we checked our background level. In some geomagnetic region, strong background continuum, presumably caused by trapped electron with energy ∼100 keV, is seen. But by cutting the high-background time-intervals, the background became significantly lower, typically with 1-3 × 10-4 counts s-1 keV-1 cm-2 (here cm2 is shown with detector geometrical area). Above 30 keV, line and continuum emission originating from activation of CdTe was significantly seen, though the level of 1-4 × 10-4 counts s-1 keV-1 cm-2 is still comparable to those seen in NuSTAR. By comparing the effective area and background rate, preliminary analysis shows that the HXI had a statistical sensitivity similar to NuSTAR for point sources, and more than twice better for largely extended sources.

    AB - Hitomi X-ray observatory launched in 17 February 2016 had a hard X-ray imaging spectroscopy system made of two hard X-ray imagers (HXIs) coupled with two hard X-ray telescopes (HXTs). With 12 m focal length, they provide fine (2′ half-power diameter; HPD) imaging spectroscopy at 5 to 80 keV. The HXI main imagers are made of 4 layers of Si and a CdTe semiconductor double-sided strip detectors, stacked to enhance detection efficiency as well as to enable photon interaction-depth sensing. Active shield made of 9 BGO scintillators surrounds the imager to provide with low background. Following the deployment of the Extensible Optical Bench (EOB) on 28 February, the HXI was gradually turned on. Two imagers successfully started observation on 14 March, and was operational till the incident lead to Hitomo loss, on 26 March. All detector channels, 1280 ch of imager and 11 channel of active shields and others each, worked well and showed performance consistent with those seen on ground. From the first light observation of G21.5-0.9 and the following Crab observations, 5-80 keV energy coverage and good detection efficiency were confirmed. With blank sky observations, we checked our background level. In some geomagnetic region, strong background continuum, presumably caused by trapped electron with energy ∼100 keV, is seen. But by cutting the high-background time-intervals, the background became significantly lower, typically with 1-3 × 10-4 counts s-1 keV-1 cm-2 (here cm2 is shown with detector geometrical area). Above 30 keV, line and continuum emission originating from activation of CdTe was significantly seen, though the level of 1-4 × 10-4 counts s-1 keV-1 cm-2 is still comparable to those seen in NuSTAR. By comparing the effective area and background rate, preliminary analysis shows that the HXI had a statistical sensitivity similar to NuSTAR for point sources, and more than twice better for largely extended sources.

    KW - active-shield

    KW - APD

    KW - BGO

    KW - CdTe-DSD

    KW - DSSD

    KW - Hard X-ray Imager

    KW - Hitomi

    KW - in-orbit performance

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